Peculiar velocities in the local Universe: comparison of different models and the implications for <i>H</i>0 and dark matter

Boruah, Supranta S.; Hudson, Michael J.; Lavaux, Guilhem

doi:10.1093/mnras/stab2320

Cited by 24 publications

(18 citation statements)

References 54 publications

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“…We calculate a posterior distribution for H 0 from the MCMC values of D. For each step in the chain, we draw a value for the peculiar velocity of the host galaxy, v pec , from a Gaussian distribution with a mean of zero and standard deviation of vpec = 600 km s −1 (e.g. Boruah et al 2021) and calculate the Hubble constant as H 0 = (zc + v pec )/D. The addition of a peculiar velocity is required because the measured redshift z is due to some combination of the expansion of the Universe and the host galaxy peculiar velocity.…”

Section: Resultsmentioning

confidence: 99%

“…Some studies using a recalibrated distance ladder without Cepheid variables have supported the larger H 0 value (Yuan et al 2019;Huang et al 2020), and others have returned an intermediate value (Freedman et al 2019;Freedman 2021). A similar story applies to constraints from strongly lensed quasars (Birrer et al 2020;Wong et al 2020) and spatially resolved nearby megamaser galaxies (Pesce et al 2020;Boruah, Hudson & Lavaux 2021). Gravitational wave sources with electromagnetic counterparts can provide precise and independent H 0 constraints in the future (Schutz 1986;Nissanke et al 2013;Abbott et al 2017) as long as enough events can be associated with a host galaxy (Feeney et al 2021).…”

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confidence: 91%

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On measuring the Hubble constant with X-ray reverberation mapping of active galactic nuclei

Ingram

Mastroserio

Klis

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We show that X-ray reverberation mapping can be used to measure the distance to type 1 active galactic nuclei (AGNs). This is because X-ray photons originally emitted from the ‘corona’ close to the black hole irradiate the accretion disc and are re-emitted with a characteristic ‘reflection’ spectrum that includes a prominent ∼6.4 keV iron emission line. The shape of the reflection spectrum depends on the irradiating flux, and the light-crossing delay between continuum photons observed directly from the corona and the reflected photons constrains the size of the disc. Simultaneously modelling the X-ray spectrum and the time delays between photons of different energies therefore constrains the intrinsic reflected luminosity, and the distance follows from the observed reflected flux. Alternatively, the distance can be measured from the X-ray spectrum alone if the black hole mass is known. We develop a new model of our reltrans X-ray reverberation mapping package, called rtdist, that has distance as a model parameter. We simulate a synthetic observation that we fit with our new model, and find that this technique applied to a sample of ∼25 AGNs can be used to measure the Hubble constant with a 3σ statistical uncertainty of ∼6 km s−1Mpc−1. Since the technique is completely independent of the traditional distance ladder and the cosmic microwave background radiation, it has the potential to address the current tension between them. We discuss sources of modelling uncertainty, and how they can be addressed in the near future.

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Section: Resultsmentioning

confidence: 99%

mentioning

confidence: 91%

On measuring the Hubble constant with X-ray reverberation mapping of active galactic nuclei

Ingram

Mastroserio

Klis

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…First, because peculiar velocities can systematically affect H 0 measurements (Boruah et al 2021;Sedgwick et al 2021), we investigate what changes in the associated uncertainty in the recession velocities have on our determination of H 0 . We find that changing the error to 150 km s −1 instead of 250 km s −1 only changes the value by 0.2% (75.3 +4.0 −3.7 km s −1 Mpc −1 ).…”

Section: Systematic Uncertaintiesmentioning

confidence: 99%

A 5% measurement of the Hubble constant from Type II supernovae

de Jaeger,

Galbany,

Riess

et al. 2022

Preprint

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The most stringent local measurement of the Hubble constant from Cepheid-calibrated Type Ia supernovae (SNe Ia) differs from the value inferred via the cosmic microwave background radiation (Planck+ΛCDM) by more than 5𝜎. This so-called "Hubble tension" has been confirmed by other independent methods, and thus does not appear to be a possible consequence of systematic errors. Here, we continue upon our prior work of using Type II supernovae to provide another, largely-independent method to measure the Hubble constant. From 13 SNe II with geometric, Cepheid, or tip of the red giant branch (TRGB) host-galaxy distance measurements, we derive H 0 = 75.4 +3.8 −3.7 km s −1 Mpc −1 (statistical errors only), consistent with the local measurement but in disagreement by ∼ 2.0𝜎 with the Planck+ΛCDM value. Using only Cepheids (𝑁 = 7), we find H 0 = 77.6 +5.2 −4.8 km s −1 Mpc −1 , while using only TRGB (𝑁 = 5), we derive H 0 = 73.1 +5.7 −5.3 km s −1 Mpc −1 . Via 13 variants of our dataset, we derive a systematic uncertainty estimate of 1.5 km s −1 Mpc −1 . The median value derived from these variants differs by just 0.3 km s −1 Mpc −1 from that produced by our fiducial model. Because we only replace SNe Ia with SNe II -and we do not find tension between the Cepheid and TRGB H 0 measurements -our work reveals no indication that SNe Ia or Cepheids could be the sources of the "H 0 tension." We caution, however, that our conclusions rest upon a modest calibrator sample; as this sample grows in the future, our results should be verified.

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“…In the following, we provide a brief description of the data used in this work. We refer readers to Boruah et al (2020Boruah et al ( , 2021 for more details on the selection and the treatment of outliers, choosing only to highlight some main features of the data sets. • A2 Supernovae: In Boruah et al (2020), we compiled the second amendment (A2) dataset of nearby supernovae from publicly available supernovae from the CfA supernovae sample (Hicken et al 2009), Carnegie Supernovae Project -Data Release 3 (CSP-DR3, Krisciunas et al 2017), the Lick observatory Supernova Survey (LOSS, Ganeshalingam et al 2013) and the Foundation sample (Foley et al 2018;Jones et al 2019) of supernovae.…”

Section: Peculiar Velocity Surveysmentioning

confidence: 99%

“…We introduced a Bayesian model comparison framework in Boruah et al (2021) to compare the performance of different velocity reconstruction models. In this model comparison framework, we look at the Bayes factor between two models, M 1 and M 2 , Bayes factor = P (D|M 1 ) P (D|M 2 ) .…”

Section: Velocity Field Comparisonmentioning

confidence: 99%

Reconstructing dark matter distribution with peculiar velocities: Bayesian forward modelling with corrections for inhomogeneous Malmquist bias

Boruah¹,

Lavaux²,

Hudson³

2021

Preprint

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We present a forward-modelled velocity field reconstruction algorithm that performs the reconstruction of the mass density field using only peculiar velocity data. Our method consistently accounts for the inhomogeneous Malmquist bias using analytic integration along the line-of-sight. By testing our method on a simulation, we show that our method gives an unbiased reconstruction of the velocity field. We show that not accounting for the inhomogeneous Malmquist bias can lead to significant biases in the forward-modelled reconstructions. We applied our method to a peculiar velocity data set consisting of the SFI++ and 2MTF Tully-Fisher catalogues and the A2 supernovae compilation, thus obtaining a novel velocity reconstruction in the local Universe. Our velocity reconstructions have a cosmological power spectrum consistent with the theoretical expectation. Furthermore, we obtain a full description of the uncertainties on reconstruction through samples of the posterior distribution. We validate our velocity reconstruction of the local Universe by comparing it to an independent reconstruction using the 2M++ galaxy catalogue, obtaining good agreement between the two reconstructions. Using Bayesian model comparison, we find that our velocity model performs better than the adaptive kernel smoothed velocity with the same peculiar velocity data. However, our velocity model does not perform as well as the velocity reconstruction from the 2M++ galaxy catalogue, due to the sparse and noisy nature of the peculiar velocity tracer samples. The method presented here provides a way to include peculiar velocity data in initial condition reconstruction frameworks.

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Peculiar velocities in the local Universe: comparison of different models and the implications for H0 and dark matter

Cited by 24 publications

References 54 publications

On measuring the Hubble constant with X-ray reverberation mapping of active galactic nuclei

On measuring the Hubble constant with X-ray reverberation mapping of active galactic nuclei

A 5% measurement of the Hubble constant from Type II supernovae

Reconstructing dark matter distribution with peculiar velocities: Bayesian forward modelling with corrections for inhomogeneous Malmquist bias

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